martin elvis, melvis@ martin elvis, [email protected] 15 years of chandra, boston, november...

Martin Elvis, [email protected] 15 Years of Chandra, Boston, November 2014

© H

arry

Mor

osz

Quasar RainChandra and the Inner Structure of AGNsWarm Absorbers, X-ray Eclipses and Broad Line Region Inflows, a unification

Martin ElvisHarvard-Smithsonian Center for Astrophysics


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arry

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osz

Chandra taught us about AGN structure

2

>100 absorption features - 6 parameter model

Chandra HETGS 850ksec spectrum of NGC 3783

AGN Wind @750 km s-1 : 2-3 phase gas in pressure equilibrium to 5%

Krongold, Nicastro, Brickhouse, Elvis, Liedahl & Mathur, 2003 ApJ 597, 832

1. X-ray Warm Absorber Outflows


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Chandra taught us about AGN structure

3

Compton ThinThickThin in 4 daysDNH>~1024cm-2 in 2 days–> ne>109 cm-3

–> R(NH) < few 1000 Rs

–> NOT the “torus” 2 days 2

days

Chandra monitoring

Risaliti et al., 2007, ApJL, 659, L111

2. Rapid eclipses by thick, cool gas clouds


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I thought I knew AGN structure

Broad Absorption LinesReflection features

Thin Vertical wind

Narrow absorption lines X-ray `warm’ absorbersBroad High ionization Emission Lines

hollow cone

Accretion disk

Supermassive black hole

X-ray/UV ionizing continuum

Accelerating bi-conical disk wind

no absorption lines

Failed Disk wind

Broad Low ionization Emission Lines

Bi-conical Extended Narrow Line Region

Elvis 2000

Disk Winds solve everything – it’s all outflows and rotation


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But…A Theory of Everything must explain

Every. Single. Thing.

Do Broad Line Region Inflows spoil it all?


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Reverberation Mapping

• d-function flash from quasar• Produces d-function response in an emission line from

a gas cloud at distance R • after “lag” time t=R/c

flux

Emission Line Response

R/c

flux

Central Continuum SourceFlash

time


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osz

Isodelay Surfaces

• Parabolas of equal delay time:

• Zero delay ONLY possible on our line-of-sight to continuum

7

= r/c

= r/c

cos1

c

r

Brad Peterson, OSU


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osz

ARP 151

Redshifts Blueshifts

Lag

time

Broad Line Region Inflows

• Velocity Resolved Reverberation Mapping (VRRM)– Bentz et al. 2010

• Redshifts at zero lag

Infall !

Redshifts at zero lag

0

Isodelay Surfaces

Peterson 2003

Infalling gasMUST be here


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osz

More blueshifts at zero lag

Broad Line Region Inflows• Inflows seem to be common

– Grier et al. 2013


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Inflow leads to disks

UMBC

• Can’t fall far without angular momentum creating a disk

• Broad Line Region is not a disk:– covers ~10% of 4p– Accretion disk covers

~0.1% of 4p .


© H

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Mor

osz

Broad Line Region Inflow

?


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Mor

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the outflow is the inflow


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Mor

osz

Can outflows solve Broad Line Region Inflows?

Use the Chandra results:

1. X-ray Warm Absorbers, Low Ionization Phase

Krongold et al. 2003

Log

Tem

pera

ture

Log Ionization parameter

2. X-ray Eclipsing Clouds

Schw

artz

child

radi

i

Density (cm-3)

X-ray Eclipsers

Elvis et al. 2004

BLR


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Mor

osz

Can outflows solve Broad Line Region Inflows?

Broad Emission Line Region

Warm Absorber (LIP)*

X-ray eclipsing clouds

Temperature T(K)

(1-2) X 10(4) Few X 10(4) <10(5)

log[Densityne (cm-3)]

8 - 10 9 - 11 9 - 10

log[Ionization parameter, U]

-1.5 – 10 -3 - -1 < 100

• Same physical conditions• Same gas?• But WA is an OUTFLOW

Outflow

* LIP = Low Ionization Phase, Krongold et al. 2003


© H

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Cool Phases in the Warm Absorber Outflow

• Found often (always?):• NCG 3783 (Krongold et al. 2003;

Netzer et al. 2003 ), • NCG 985 (Krongold et al. 2005b ,

2009 ), • NGC 4051 (Krongold et al.

2007 ), • Mrk 279 (Fields et al. 2007 ), • NGC5548 (Andráde-Velasquez et

al. 2010) 9Z

Thermal equilibrium

Log(1/Pressure)

Log(

Tem

pera

ture

)Form naturally in gas illuminated

by quasar spectrum – Krolik, McKee & Tarter 1981; Chakravorty+08,09

• High metallicity helps -- Chakravorty et al. 2012


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Cool Phase is dense

• 100 x denser than Warm Absorber: ne ~ 108 cm-2

• Column Density, NH ~ 30 x NH(WA) ≤ 1024 cm-2

• Size, d ~ 1016 cm ≈ 300 M8 Rg ≈ 60 RX-ray(M8)• Hard to accelerate• High Mass/cross-section ratio

– Mushotzky, Solomon & Strittmatter 1972– Risaliti & Elvis 2010

• Stops accelerating while warm phase continues up to escape velocity?


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osz

Dense condensed phase, below vescape

Falls back after ~1 dynamical time ~ 1 year

= Quasar Rain


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Quasar Rain: How quickly does it form?• Cooling time:• tcool = 1.8x1010 L0(T)/L(T) T6

1/2 ne8-1 sec.

– L(T) ~60 L0(T) Tucker 1975, Gehrels & Williams 1993

• tcool = 3 T61/2 ne8

-1 days ≈ 3 days

• Collapse time:• tsound = cs/R = 300 km s-1 / 1012.5 cm ≈ 23 days


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Mor

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How quickly does wind reach vescape?

• Acceleration time to vescape:

• tacc ~ 4M8 days (Risaliti & Elvis 2010 model)

• tcool < tacc < tsound

• Similar ballpark – competitive processes• Some condensations escape, some fall back


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Mor

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Fate of the infalling rain?

• Feels ram pressure of warm outflowing gas

• Mach ~20• Strips away gas into a tail• “raindrops” destroyed• On elliptical orbits• Non-radial tails


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We see these ablating “raindrops”• NGC1365 X-ray eclipsing clouds• NH rises fast at low covering

factor, fc

• Then NH drops as fc increases• “Cometary” tail – non-radial• Lifetime ~60 days• Cannot reach high infall velocity

Maiolino et al. 2012

Cove

ring

fact

orN

H

1 day


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Quasar Rain

• Explains:– Infalling Broad Line Region Gas– at moderate infall velocities

• Unifies: – Broad Line Region clouds– Low Ionization X-ray Warm Absorber– X-ray eclipsing clouds– Cometary tails on X-ray eclipsing clouds

• Forms naturally• Appealing: Disk winds still solve everything


© H

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The Way Forward

Vikhlinin et al. 2013

×100Chandra gratings

10

0.2 0.5

Chandra HRC-LETGS

>250 X Chandra

CalorimeterA(0.5)~10,000cm2

700 X ChandraNGC3783 in 1ksec

dE ~< 5 eVR>~100 @ 0.5keVSimilar to Athena

R ~ 5000>10 X Chandra

NGC3783 spectrum in 3 ksecVariability -> density, radiusLarge Surveys: M, L/LEdd, …High z

60 km s-1

Resolves thermal line widthsTurbulence, Tthermal vs Tion

Curve of growth n(ion)Diagnostic line ratiosResolves UV-like components

Nearer term: “ARCUS” – see Randall Smith poster 8.11


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Quasar Rain/Virga• Explains:

– Infalling Broad Line Region Gas– at moderate infall velocities

• Unifies Chandra and reverberation results: – Broad Line Region clouds– Low Ionization X-ray Warm Absorber– X-ray eclipsing clouds– Cometary tails on X-ray eclipsing clouds

• Forms naturally• Appealing: Disk winds still solve everything

KWWL.com

martin elvis, melvis@ martin elvis, [email protected] 15 years of chandra, boston, november...

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